In the model of magnetospheric accretion, it is proposed that the inner gaseous disk is truncated by the strong stellar magnetic field because of the magnetic pressure exerted perpendicular to the magnetic field lines threading the disk. Thus, a region of a few stellar radii surrounding the star is formed where the disk plane is almost completely evacuated from gas particles [1]}. Instead of further spiralling inwards, the gas particles can only move freely along the field lines, which effectively serve as funnels that channel the gas onto the star. As the gas impacts the stellar surface at high latitudes, it creates heated shock regions close to the poles [2]}.
